The probability of identifying CVs within SDSS if their optical emission is dominated by the luminosity of the accretion-heated WD as a function of M_wd. From top to bottom: the effective temperature calculated using Eq. (1) in Townsley & Gänsicke (2009); R_wd²; the absolute i-band magnitude; the minimum and maximum distance at which SDSS will have obtained follow-up spectroscopy; the effective survey volume for a spherical cap with b > 30°, H_z = 200 pc, and d_min < d < d_max, and the relative probability normalized to M_wd = 0.6 M_⊙. Three secular mean accretion rates are shown,  ⟨ Ṁ ⟩  = 3  ×  10^-11   M_⊙   yr^-1 (solid lines), 10^-10   M_⊙   yr^-1 (dotted lines), and 3  ×  10^-10   M_⊙   yr^-1 (dashed lines).